how energy becomes matter: emc2: probing qgp with...

How Energy Becomes Matter: E ⇒ mc2:Probing QGP with Strangeness

Jan RafelskiDepartment of Physics, The University of Arizona, Tucson, AZ 85721

Seminar at IFJ, Krakow July 3, 2018How is matter produced in the form we are familiar with? This question and theanswer were formulated more than half a century ago when Big-Bang modelbecame the new paradigm. The entire relativistic heavy ion collision researchprogram was build to experimentally confirm theory. ALICE is the experimentat the CERN LHC build predominantly to study how energy turns into matterin ultra relativistic nuclear (AA) collisions. In contemporary experiments keyinformation is derived in study of multistrange hadrons which carry informationboth, about the process of matter production (hadronization) E ⇒ mc2, as wellas about earlier stages when entropy and strangeness are produced. Veryrecent results show that even a relatively small pp and pA collisions at theLHC energy-scale are creating the new quark-gluon plasma (QGP) phase ofmatter.

Jan Rafelski-Arizona: IFJ-Krakow,July 3,2018 () Universe & Strangeness 1 / 64

Background: 1992 NATO School Il Ciocco Poster


1965-7 – Hagedorn’s singular Statistical Bootstrap

accepted as ‘the’ initial singular hot Big-Bang theory

Boiling Primordial Matter Even though no one was present when the Uni-verse was born, our current understanding of atomic, nuclear and elementaryparticle physics, constrained by the assumption that the Laws of Nature areunchanging, allows us to construct models with ever better and more accuratedescriptions of the beginning.. . . We would have never understood these thingsif we had not advanced on Earth the fields of atomic and nuclear physics. Tounderstand the great, we must descend into the very small.


1966-1968: SBM Hot Big-Bang via Hagedornbecomes conventional wisdom

1965 (Bootstrap year): Penzias and Wilson discover CMB1966-1968: Hot Big-Bang becoming conventional wisdom

“We did NOT know what was there at the ‘Beginning’how matter was created.”


I will (mostly) talk about these itmes

50+ years ago particle production in pp reactions prompted introductionof Hagedorn Temperature TH along with singular energy density – bothlinked to the Big-Bang.By 1980 TH reinterpreted as the critical temperature at which vacuum‘melts’, matter surrounding us dissolves; This prompts CERN and BNLexperimental relativistic heavy ion collision program to recreatequark-gluon-plasma (QGP) pre-matter in laboratory.We developed laboratory observables of this quark-gluon phase ofmatter: cooking strange quark flavor.18-13 years ago we witnessed both CERN and BNL announcing thediscovery of QGP prompting models of the properties of the babyUniverse 10 ns – 18µs.We develope detailed understanding how matter in Universe emergesfrom energy E ⇒ mc2: statistical hadronization model (SHM).Understanding of early Universe allows consistency studies: we setlimits on variation of natural constants in early Universe, constrain anynew radiance (darkness); characterize cosmic microwave neutrinos.Interface to vacuum bi-stability issue.


For many details I recommend reading the text books


Quarks make pions (mesons); squeeze many together

In the early Universe the building blocks of baryons and mesons wereliberated: Universe was made from a new type of matter: QGP


Can we recreate Big-Bang in lab?

Relativistic Heavy Ion CollisionsUniverse time scale 18 ordersof magnitude longer, henceequilibrium of leptons &photonsBaryon asymmetry six ordersof magnitude larger inLaboratory, hence chemistrydifferentUniverse: dilution by scaleexpansion, Laboratoryexplosive expansion of afireball

=⇒ Theory connects RHI collision experiments to Universe


First question; is there really a fireball of matter?Two extreme views on stopping in RHI collisionsFly-through full stopping

Transparency ⇐Two opposite views⇒ SPS-RHIC large stoppingLHC a nice fireball in all casesCitations favor wrong paper: 272 vs 239 today


My views about importance of RHI collisions & Quark GluonPlasma?

1 RECREATE THE EARLY UNIVERSE IN LABORATORYRecreate and understand the high energy density conditions prevailingin the Universe when matter formed from elementary degrees offreedom (quarks, gluons) at about 20 µs after the Big-Bang.

2 PROBING OVER A ‘LARGE’ DISTANCE THE (DE)CONFININGQUANTUM VACUUM STRUCTUREThe quantum vacuum, the present day relativistic æther, determinesprevailing form of matter and laws of nature.

3 STUDY OF THE ORIGIN OF MATTER & OF MASSMatter and antimatter created when QGP ‘hadronizes’. Mass of matteroriginates in the confining vacuum structure

4 PROBE ORIGIN OF FLAVORNormal matter made of first flavor family (d, u, e, [νe]). Strangeness-richquark-gluon plasma the sole laboratory environment filled ‘to the rim’with 2nd family matter (s, c, [µ, νµ])). and considerable abundance of band even t.

5 PROBE STRONGEST FORCES IN THE UNIVERSEFor a short time the relativistic approach and separation of large chargesZe↔ Ze generates EM fields 1000’s time stronger than those inMagnetars; strongfields=strong force=strong acceleration=acceleration frontier


At CERN: Strangeness a popular QGP signatureI argued 1980-81 that anti-strangeness in QGP can be more abundant thananti-light quarks. Many experiments followed.

A: There are many strange particles allowing to studydifferent physics questions (q = u, d):

K(qs), K(qs), K∗(890), Λ(qqs), Λ(qqs), Λ(1520)

φ(ss), Ξ(qss), Ξ(qss), Ω(sss), Ω(sss)

B: Production rates hence statistical significance is high.C: Strange hadrons are subject to a self analyzing decay


The idea of 1980 in detail:CERN-TH-2969 of October 1980; Published

in “Statistical Mechanics of Quarks and Hadrons”, H. Satz, editor,

Elsevier 1981; Also other conferences 1980 incl Quark Matter I

Who says there is chemical equilibrium in QGP? (Biro-Zimanyi)Jan Rafelski-Arizona: IFJ-Krakow,July 3,2018 () Universe & Strangeness 13 / 64

....till today we live with some consequences


Instant success of strangeness signature proposal


Strange hadrons from QGP: two-step formation mechanism1 GG→ ss (thermal gluons collide)

GG→ cc (initial parton collision)gluon dominated reactions

2 hadronization of pre-formeds, s, c, c, b, b quarks

Evaporation-recombination formation of complex rarely produced (multi)exoticflavor (anti)particles from QGP is signature of quark mobility thus ofdeconfinement. Enhancement of flavored (strange, charm,. . . ) antibaryonsprogressing with ‘exotic’ flavor content. J. Rafelski, Formation andObservables of the Quark-Gluon Plasma Phys.Rept. 88 (1982) p331; P.Koch, B. Muller, and J. Rafelski; Strangeness in Relativistic Heavy IonCollisions, Phys.Rept. 142 (1986) p167


Anticipated: Sudden hadronization of QGPProposed evidence: matter-antimatter symmetry


Pb-Pb SPS collisions also show matter-antimattersymmetry


Anticipated: Central QGP fireballProposed evidence: (Strange)Antimatter


NA49 Pb-Pb SPS confirmation Λ/p > 1 (1980prediction)


Predicted: Strange antibaryons enhancedWA97 SPS Antihyperons: The largest observed QGP medium effect

Enhancement GROWS with a) strangeness b) antiquark content as wepredicted. Enhancement with respect to yield in p–Be collisions, scaled up with thenumber of ‘wounded’ nucleons. Result→ CERN QGP discovery announcementin 2000. All other CERN strangeness experimental results agree.


Today: Effect remains largest medium effect in RHI collisions


Reminder: When and how did we discover QGP?


Current interest in small systems: Strange antibaryonenhancement smoothly rising with entropy of fireball


Small systems: Ξ(ssq) Alice 2014 needs minor attention


Small system: particle yield constrained by conservation law:Canonical phase space required


Small system: An elegant nonabelian group theory approach


.... and the strangeness part is REDISCOVERED decade later


Strangeness conservation alone: in QGP book JL/JR; p225-232:1-2-3-strange flavored particle suppression factors

〈NCEκ 〉 = NGC

κ

Iκ(2NGCpair)

I0(2NGCpair)

.

Canonical yield-suppression factors Iκ/I0 as function of the grand-canonicalpair yield N. Short-dashed line: the suppression of triply-strange-flavoredhadrons; long-dashed line: the suppression of doubly-strange-flavoredhadrons; and solid line, the suppression of singly-strange-flavored hadrons.


Ξ(ssq)/φ(ss) (nearly) constant: same production mechanism

M. Petran, J. Rafelski, Multistrange Particle Production and theStatistical Hadronization Model Phys.Rev. C 82 (2010) 011901


The chemical hadronization analysisfrom (re)invention to generalization

Magic coincidence: while we battled our referee for 6 months KrzysztofRedlich enters this field with the 2 page preprint in August 1998:Unified description of freezeout parameters in relativistic heavy ioncollisions, Phys.Rev.Lett. 81 (1998) 5284-5286


Chemical reactions involving quarks


WHY STATISTICAL HADRONIZATION MODEL. . . (SHM) WORKS

a) Confinement: =⇒ breakup into free quarks not possible;b) Strong interaction: =⇒ equal hadron production strength irrespective ofproduced hadron type=⇒ ‘elementary’ hadron yields depend only on the available phase spaceHistorical approaches:

Fermi: Micro-canonical phase spacesharp energy and sharp number of particles

E. Fermi, Prog.Theor.Phys. 5 (1950) 570: HOWEVERExperiments report event-average rapidity particle abundances,model should describe an average event

Canonical phase space: sharp number of particlesensemble average energy E → T temperatureT could be, but needs not to be, a kinetic process temperature

Grand-canonical – ensemble average energy and number of particles:N → µ ⇔ Υ = e(µ/T)

Our interest: bulk QGP fireball properties of hadron source evaluatedindependent of complex explosion dynamics =⇒ analyze integratedhadron spectra.


SHARE Idea/Team: US-Polish NATO collaboration 2002/04Statistical HAadronization with REsonances


Examples SHM Analysis (Chemical Nonequilibrium)

Particle Yield Example:LHC

M. Petran, J.Letessier, V. Petracek, J. Rafelski Phys.Rev.C 88 (2013) no.3, 034907

Bulk properties from SHM yields

J. Letessier, J. Rafelski, Eur.Phys.J. A 35 (2008) 221-242


SHM fit Quality LHC Pb-Pb 2.76 TeV data


SHARE consistent with lattice QCDChemical nonequilibrium + supercooling= sudden fireball breakup


SPS, RHIC, LHC AA SHM Digest

Strange antibaryon signature of QGP leads to discovery ofuniversal properties of QGP at hadronization; differences in:Volume size, Strangeness saturation.Universality of fireball bulk properties across the entire reactionenergy domain we express in terms of the invariant measure

At SPS, RHIC: Baryon number deposition varies strongly asfunction of collision energy. This is the chemical potentialdependence on collision energy. WHY? – To clarify question: whythere is no McLerran-Bjorken transparency?


Smaller systems hadronize earlier (more dense fireball)


A few first look at small ALICE systems remarks

ALICE small system results shows growth γs of strangeness yield withsize of the system.

Hadronization condition T a few MeV higher compared to large systems:conclusion there is less/no supercooling in less explosive expansion.

Corresponding bulk matter properties are higher. No test of universalhadronization / conformal anomaly was as yet performed.

Small system net flavor content universally zero (and it seems we aresensitive due to small system): there is no electric charge, etc.

There is no doubt that after 38 years of waiting the pp→ AA ALICEresults demonstrate that there are 10-20-30% canonical phasespace effects: when strange pairs are few and baryon number israre, strange antibaryons are slightly suppressed as the correcttheory predicts. Dominant effect still from strangeness chemicalnon-equilibrium γs . No publication forthcoming as lack ofresources prevents appropriate analysis effort.


Summary: In last 100 years (variant of A Bialas fest slide)Particle accelerators barely started 100 years ago, particleproduction study begins in earnest 75 years ago; leadingus to understand origin of mass of matter, the earlyUniverse, the Æther = quantum vacuum, and how energybecomes matter in primordial Universe E → mc2.

Much ‘naive’ and ‘profound ’ mystery remains: Whycolliding hadrons make lots of entropy – what else is inquantum vacuum? . . .

Krakow coffee houses, Zakopane mountains: These areessential tools assuring future progress and continuedsuccess for the large Krakow group that rose to Worldprominence in the past 50 years.

Big riddles: In my view the new physics we are lookingfor is associated with ‘FORCES’ and the biggesthammer is a relativistic heavy ion, side perhaps ofsome laser stuff


A quick look at: Explore the Universe: today← QGP

The Universe Composition in Single View

dark energy matter radiation ν, γ BBN+leptons hadronsDifferent dominance eras: Temperature grows to right


Objective: connect the hot Hagedorn Universe with present day

The contents of the Universe today(fractions change ‘rapidly’ in expanding Universe)

1. Visible (baryonic) matter(less 5% of total energy inventory)

2. Free-streaming matteri.e particles that do not interact – have ‘frozen’ out:

photons: since T = 0.25eV (insignificant in inventory)neutrinos: since T = 1.5–3.5 MeV (insignificant)dark matter (25% in energy inventory)

1 Massive ColdDarkMatter from way before QGP hadronization2 massless dark matter: darkness: maybe ‘needed’, origin precedes

neutrino decoupling

3. Dark energy = vacuum energy (70% of energy inventory)

darkness: quasi-massless particles influence early Universe dynamics


Particle composition in thermal Universe

The chemistry of particle reactions in the Universe has three ‘chemical’potentials needing to be constrained. There are also three physicsconstraints Michael J. Fromerth, JR etal e-Print: astro-ph /0211346;arXiv:1211.4297→ Acta Phys.Polon. B43 (2012), 2261

i. Electrical charge neutrality

nQ ≡∑

Qi ni(µi,T) = 0,

Qi and ni charge and number density of species i.

ii. Net lepton number equals(?) net baryon numberB/L-asymmetry can hide in neutrino-antineutrino imbalance

iii. Prescribed value of entropy-per-baryon ≡ nB/nγ

σ

nB≡

∑i σi(µi,T)∑

i Bi ni(µi,T)= 3.2 . . . 4.5× 1010

S/B ' 3–5×1010, results shown for 4.5× 1010


Particle composition: balancing ‘chemical’ reactions

=⇒ Antimatter annihilates to below matter abundance beforeT = 30 MeV, universe dominated by photons, neutrinos, leptons forT < 30 MeV


Mechanisms assuring hadrons in thermal equilibrium

The key doorway reaction to abundance (chemical) equilibrium of the fastdiluting hadron gas in Universe:

π0 ↔ γ + γ

The lifespan τπ0 = 8.4× 10−17 sec defines the strength of interaction whichbeats the time constant of Hubble parameter of the epoch. Inga Kuznetsovaand JR, Phys. Rev. C82, 035203 (2010) and D78, 014027 (2008)(arXiv:1002.0375 and 0803.1588).Equilibrium abundance of π0 assures equilibrium of charged pions due tocharge exchange reactions; heavier mesons and thus nucleons, and nucleonresonances follow:

π0 + π0 ↔ π+ + π−. ρ↔ π + π, ρ+ ω ↔ N + N, etc

The π0 remains always in chemical equilibrium All charged leptons always inchemical equilibrium – with photonsNeutrinos freeze-out at T = O2-4MeV, more discussion followsPhotons freeze-out at T = 0.25 eV

But is the early Universe really made of hadrons?


Free streaming matter not same as thermal matter

Free-streaming matter in the Universe: solution of kinetic equations withdecoupling boundary conditions at Tk (kinetic freeze-out).

ρ =g

2π2

∫ ∞0

(m2 + p2

)1/2p2dp

Υ−1e√

p2/T2+m2/T2k + 1

, P =g

6π2

∫ ∞0

(m2 + p2

)−1/2p4dp

Υ−1e√

p2/T2+m2/T2k + 1

,

n =g

2π2

∫ ∞0

p2dp

Υ−1e√

p2/T2+m2/T2k + 1

.

These differ from the corresponding expressions for an equilibriumdistribution by the replacement m→ mT(t)/Tk only in the exponential.Only for massless photons free-streaming = thermal distributions (absence ofmass-energy scale). For CDM (cold dark matter) mCDM >> Tk; for neutrinosmν << Tk.


C. Cercignani, and G. Kremer. The Relativistic Boltzmann Equation: Basel, (2000).H. Andreasson, “The Einstein-Vlasov System”Living Rev. Rel. 14, 4 (2011) Y. Choquet-Bruhat.General Relativity and the Einstein Equations, Oxford (2009).

Distinct Composition Eras in the Universe

Composition of the Universe changes as function of T:From Higgs freezing to freezing of QGPQGP hadronizationHadronic antimatter annihilationOnset of neutrino free-streaming just before and whene+e− annihilate; overlapping with begin ofBig-Bang nucleosynthesis within a remnant e+e− plasmaRadiation ‘Desert’(ν, γ)emergence of free streaming dark matterPhoton Free-streaming (CMB) – Composition Cross-Pointemergence of Dark energy = vacuum energy


Count of Degrees of Freedom

Distinct Composition Eras visible. Equation of state from lattice-QCD, and at high T

thermal-QCD must be used [1,2].


[1] S. Borsanyi, Nucl. Phys. A904-905, 270c (2013)[2] Mike Strickland (private communication of results and review of thermal SM).

Reheating

Once a family ‘i’ of particles decouples at a photon temperature of Ti, adifference in its temperature from that of photons will build up duringsubsequent reheating periods as other particles feed their entropy intophotons. This leads to a temperature ratio at Tγ < Ti of

R ≡ Ti/Tγ =(

gS∗(Tγ)

gS∗(Ti)

)1/3

.

This determines the present day reheating ratio as a function ofdecoupling temperature Ti throughout the Universe history.Example: neutrinos colder compared to photons.Reheating ‘hides’ early freezing particles: darkness


Connecting Universe age to temperatureFriedmann−Lemaitre−Robertson−Walker (FRW) cosmology

Einstein Universe:

Gµν = Rµν −(

R2

+ Λ)

gµν = 8πGNTµν ,

where Tµν = diag(ρ,−P,−P,−P), R = gµνRµν , and• Homogeneous and • Isotropic metric

ds2 = gµνdxµdxν = dt2 − a2(t)[

dr2

1− kr2 + r2(dθ2 + sin2(θ)dφ2)].

a(t) determines the distance between objects comoving in theUniverse frame. Skipping gµν → Rµν

Flat (k = 0) metric favored in the ΛCDM analysis, see e.g. PlanckCollaboration, Astron. Astrophys. 571, A16 (2014)[arXiv:1303.5076] and arXiv:1502.01589 [astro-ph.CO]].


Definitions: Hubble parameter H and deceleration parameter q:

H(t) ≡ aa

; q ≡ −aaa2 = − 1

H2aa,⇒ H = −H2(1 + q).

Two dynamically independent Einstein equations arise

8πGN

3ρ =

a2 + ka2 = H2

(1 +

ka2

),

4πGN

3(ρ+ 3P) = − a

a= qH2.

solving both these equations for 8πGN/3→ we find for the decelerationparameter:

q =12

(1 + 3

Pρ

)(1 +

ka2

); k = 0

In flat k = 0 Universe: ρ fixes H; with P also q fixed, and thus also Hfixed so also ρ fixed, and therefore also for ρ = ρ(T(t)) and also Tfixed. Knowing the Universe composition in present era we canintegrate back IF we know what is the contents.


Evolution Eras and Deceleration Parameter q

Using Einsteins equations solving for GN = GN

q ≡ − aaa2 =

12

(1 + 3

Pρ

)(1 +

ka2

)k = 0 favored

Radiation dominated universe: P = ρ/3 =⇒ q = 1.

Matter dominated universe: P ρ =⇒ q = 1/2.

Dark energy (Λ) dominated universe: P = −ρ =⇒ q = −1.Accelerating Universe


‘Recent’ evolution

Evolution of temperature T and deceleration parameter q fromnear/after BBN to the present day: time grows to right


Long ago: Hadron and QGP Era

QGP era down to phase transition at T ≈ 150MeV. Energy densitydominated by photons, neutrinos, e±, µ± along with u, d, s quarks.2 + 1-flavor lattice QCD equation of state usedu, d, s,G lattice energy density is matched by ideal gas of hadronsto sub percent-level at T = 115MeV.Hadrons included: pions, kaons, eta, rho, omega, nucleons, delta,hyperonsPressure between QGP/Hadrons is discontinuous (need mixedphase) hard to notice discontinuity in q (slopes match). A firststudy, better EOS can be used.


From QGP across BBN

Temperature T and deceleration parameter q from QGP era until near BBN. Timegrows to right


EW and QGP Eras

Temperature T and deceleration parameter q from Electro-Weak symmetric era tonear QGP hadronization. Time grows to right


What is this all good for? A few examples

‘Darkness’ in the Universe enters laboratory experiments



Time independence of natural constants



Knowing neutrino microwave background – look for them



Attempts to understand Universe bi-stability



EOS with free-streaming massive neutrinos


Summary Cosmo

50 years ago particle production in pp reactions prompted introduction ofHagedorn Temperature TH along with singular energy density – linked tothe Big-Bang;By 1980 TH critical temperature at which vacuum ‘melts’, mattersurrounding us dissolves; This prompts CERN and BNL experimentalprogram to recreate pre-matter in laboratory.Today: In laboratory: We explore the phase diagram of QGP; Incosmology: we study the evolution of the Quark-Universe across manydomains to the present day.We have detailed understanding how Hot Hagedorn Universe evolvesand the matter in Universe arisesComprehensive view allows diverse consistency studies: we set limitson variation of natural constants in early Universe, constrain any newradiance (darkness); characterize cosmic microwave neutrinos. Interfaceto vacuum bi-stability issue.


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